
Atmospheric Imaging Assembly (AIA): AIA provides multiple high resolution full-disk image of the solar corona and transition region upto 0.5 R\(_\odot \)  of the solar limb with spatial resolution of pixel size 0\(.\!\!^{\prime \prime }\)6 and temporal resolution of 12 second. It consists of four generalised Cassegrain telescopes with a 20 cm primary mirror and an active secondary mirror on each telescope. Each of the four telescope has a field of view (FOV) of \(\approx \)  41 \(\mbox{$~\!\!^{\prime }$}\)  circular diameter and observes the full-disk over a 4k \(\times \)  4k CCD.
<FIGURE><TABLE><FIGURE>A guiding telescope is mounted on the side of the telescope tube with an achromatic refractor, a band-pass entrance filter focused at 5700 Å, and a Barlow-lens assembly. To provide the low thermal coefficient of thermal expansion, the telescope mirrors are fabricated on zerodur substrates. AIA provides seven the information of the solar surface in seven EUV and three UV channels. The seven EUV bands are centered at different lines emitting at different temperatures from 335 Å (Fe XVI), 304 Å (He II, T\(\sim \) 0.05 MK), 171  Å (Fe IX, T \(\sim \) 0.6 MK), and 193  Å (Fe XII, T \(\sim \) 0.6 MK) to hotter temperatures of 94  Å (Fe XVIII, T\(\sim \) 6.3 MK), 131 Å (T\(_1\) = 10 MK and T\(_2\) = 0.64 MK), and 211  Å (T\(_1\)  \(\sim \)  20 MK and T\(_2\)  \(\sim \) 1.6 MK).
Two UV wavebands are centered at 1600 Å (C IV), 1700 Å, and 4500 Å (continuum).
Responses to different solar emissions in the AIA instrument can compute with with the CHIANTI solar spectral model ([1]}). The response function curve for the six EUV wavebands are dominated by iron emission lines and are presented in Figure REF . A comparative and detail description of these UV and EUV channels is presented in table REF . The temperature for different wavebands varies from 6\(\times \) 10\(^4\)  K to 2\(\times \) 10\(^7\)  K.
The multi-wavelength observations from the AIA instrument in UV and EUV channels are presented in Figure REF .

Helioseismic and Magnetic Imager (HMI):
HMI is focused to map the magnetic fields and velocity fields at the solar surface and use to probe the oscillations at the photosphere with 6173 Å Fe I absorption line. It measures the Dopplershifts to determine the surface velocity at the photosphere and creates a fulldisk Dopplergram with a temporal resolution of 45 second and pixel size of 0\(.\!\!^{\prime \prime }\)5. These Dopplergrams (maps of solar surface velocity) are important to study the interior of the Sun.
HMI contains an optics package, an electronics box, and a harness to connect both of them. Optical package ensembles a front-window filter, a telescope, waveplates for polarimetry , one blocking filter, an image stabilization system, five stage Lyot filter, two wide field tunable Michelson interferrometers, and a pair of 4k \(\times \)  4k cameras. The Lyot filter is based on the same basic design as of Michelson Doppler Imager [2]}.
The fulldisk longitudinal magnetic field are measured using the Zeeman effect with the splitting of the spectral lines.
<TABLE>For the magnetic field extrapolations and more precise magnetic field observations, the Space-weather HMI Active Region Patches (SHARPs) data is used. The detail analysis of HMI SHARP data is given by [3]}. This SHARP data series is centered to characterize the distribution of magnetic field and focused on a small spatial scale. Thus the SHARP data provides a deviation from the global/potential magnetic field configuration. SHARP follow and automatically detect each single AR patch of solar magnetic field during its complete life cycle from appearance on the solar disk to disappearance ([4]}). This SHARP data series provide indices, photospheric vector magnetic field data maps of Doppler velocity, maps of continuum intensity, LOS magnetic field and other variables. This SHARP data is available for the individual AR on the solar disk with 12 minute cadence and the real time parameter source are given in table REF .

<FIGURE>